Observation of an outburst of the transient X-ray pulsar A0535+26 in 1980
著者
和文:
Nagase, F.,
Hayakawa, S.,
Kunieda, H.,
Makino, F.,
Masai, K.,
Tawara, Y.,
Inoue, H.,
河合 誠之,
Koyama, K.,
Makishima, K.,
Matsuoka, M.,
Murakami, T.,
Oda, M.,
Ogawara, Y.,
Ohashi, T.,
Shibazaki, N.,
Tanaka, Y.,
Miyamoto, S.,
Tsunemi, H.,
Yamashita, K.,
Kondo, I..
英文:
Nagase, F.,
Hayakawa, S.,
Kunieda, H.,
Makino, F.,
Masai, K.,
Tawara, Y.,
Inoue, H.,
Kawai, N.,
Koyama, K.,
Makishima, K.,
Matsuoka, M.,
Murakami, T.,
Oda, M.,
Ogawara, Y.,
Ohashi, T.,
Shibazaki, N.,
Tanaka, Y.,
Miyamoto, S.,
Tsunemi, H.,
Yamashita, K.,
Kondo, I..
言語
English
掲載誌/書名
和文:
英文:
Astrophysical Journal
巻, 号, ページ
Vol. 263
pp. 814-822
出版年月
1982年12月
出版者
和文:
英文:
会議名称
和文:
英文:
開催地
和文:
英文:
アブストラクト
X-ray observations of the pulsar A0535+26 by the Hakucho satellite are analyzed for evidence of a pulse change period. The scanning was carried out in the energy ranges 1-9 keV and 9-22 keV. A pulse arrival time analysis was carried out, resulting in an estimate of a 40 day orbital period, within the 90% confidence interval. The daily average pulse period decreased gradually from 103.67 to 103.61 sec during the 12-day observation period. An upper limit of nearly 120 days was set on the orbital period after consideration of the mass function. It is suggested that the pulse period change observed can be accounted for by a steady decrease in the intrinsic period at a rate proportional to a diminishing luminosity. Furthermore, the outbursts may occur during periastron passage in a highly eccentric orbit, thus explaining the transience of the X-ray source A0535+26.
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